Direct collapse black hole formation from synchronized pairs of atomic cooling haloes

Visbal, Eli; Haiman, Zoltán; Bryan, Greg L.

doi:10.1093/mnras/stu1794

Cited by 127 publications

(133 citation statements)

References 42 publications

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“…In the Rarepeak region, which has a volume of 133.6 cMpc 3 , we find 5 synchronised pairs. Given the difference in volume our abundance is higher by a factor of approximately 5 compared to that of Visbal et al (2014b). However, the Rarepeak region represents an over-density of approximately 1.7 compared to an average region of the universe and Visbal et al were unable to account for metal enrichement in their analysis which may have a led to an over-estimate of the number density of synchronised halo candidates in that case.…”

Section: Synchronised Haloesmentioning

confidence: 84%

The emergence of the first star-free atomic cooling haloes in the Universe

Regan

Wise

O’Shea

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Using the Renaissance suite of simulations we examine the emergence of pristine atomic cooling haloes that are both metal-free and star-free in the early Universe. The absence of metals prevents catastrophic cooling, suppresses fragmentation, and may allow for the formation of massive black hole seeds. Here we report on the abundance of pristine atomic cooling haloes found and on the specific physical conditions that allow for the formation of these directcollapse-black-hole (DCBH) haloes. In total in our simulations we find that 79 DCBH haloes form before a redshift of 11.6. We find that the formation of pristine atomic haloes is driven by the rapid assembly of the atomic cooling haloes with mergers, both minor and/or major, prior to reaching the atomic cooling limit a requirement. However, the ability of assembling haloes to remain free of (external) metal enrichment is equally important and underlines the necessity of following the transport of metals in such simulations. The candidate DCBH hosting haloes we find, have been exposed to mean Lyman-Werner radiation fields of J LW ∼ 1 J 21 and typically lie at least 10 kpc (physical) from the nearest massive galaxy. Growth rates of the haloes reach values of greater than 10 7 M per unit redshift, leading to significant dynamical heating and the suppression of efficient cooling until the halo crosses the atomic cooling threshold. Finally, we also find five synchronised halo candidates where pairs of pristine atomic cooling haloes emerge that are both spatially and temporally synchronised.

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Section: Synchronised Haloesmentioning

confidence: 84%

The emergence of the first star-free atomic cooling haloes in the Universe

Regan

Wise

O’Shea

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…5. However, if we now use a collapse time of 10 Myr, as suggested by Visbal, Haiman & Bryan (2014), for the same J LW,crit = 30, we find: 1 halo at z = 10.1 with Z < 10 −3.5 Z , 3 regions at z = 9.00 (all with Z = 0), 6 regions at z = 8.09 (3 regions with Z = 0, and 3 regions with Z < 10 −3.5 Z ), 17 regions at z = 7.33 (7 regions with Z = 0, and 10 regions with Z < 10 −3.5 Z ). All the regions are in halos with M h > 10 8 M .…”

Section: Number Density Of Direct Collapse Regions In Chunkymentioning

confidence: 99%

On the number density of ‘direct collapse’ black hole seeds

Habouzit¹,

Volonteri²,

Latif³

et al. 2016

Mon. Not. R. Astron. Soc.

145

183

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Supermassive black holes (BHs) of millions solar masses and above reside in the center of most local galaxies, but they also power active galactic nuclei and quasars, detected up to z = 7. This observational evidence puts strong constraints on the BH growth and the mass of the first BH seeds. The scenario of "direct collapse" is very appealing as it leads to the formation of large mass BH seeds in the range 10 4 − 10 6 M , which eases explaining how quasars at z = 6−7 are powered by BHs with masses > 10 9 M . Direct collapse, however, appears to be rare, as the conditions required by the scenario are that gas is metal-free, the presence of a strong photo-dissociating Lyman-Werner flux, and large inflows of gas at the center of the halo, sustained for 10 − 100 Myr. We performed several cosmological hydrodynamical simulations that cover a large range of box sizes and resolutions, thus allowing us to understand the impact of several physical processes on the distribution of direct collapse BHs. We identify halos where direct collapse can happen, and derive the number density of BHs. We also investigate the discrepancies between hydrodynamical simulations, direct or post-processed, and semianalytical studies. We find that for direct collapse to account for BHs in normal galaxies, the critical Lyman-Werner flux required for direct collapse must be much less than predicted by 3D simulations that include detailed chemical models. However, when supernova feedback is relatively weak, enough direct collapse BHs to explain z = 6 − 7 quasars can be obtained for more realistic values of the critical Lyman Werner flux.

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“…Another possibility is more massive BH seeds with ∼ 10 3 − 10 5 M formed by direct collapse of supermassive stars in protogalaxies (e.g., Loeb & Rasio 1994;Oh & Haiman 2002;Bromm & Loeb 2003;Begelman et al 2006;Regan & Haehnelt 2009a,b;Hosokawa et al 2012Hosokawa et al , 2013Inayoshi et al 2014;Visbal et al 2014;Inayoshi & Tanaka 2015;Chon et al 2016;Regan et al 2016a,b;Hirano et al 2017;Inayoshi et al 2018) and runaway stellar collisions (e.g., Omukai et al 2008;Devecchi & Volonteri 2009;Katz et al 2015;Yajima & Khochfar 2016;Stone et al 2017;Sakurai et al 2017;Reinoso et al 2018). Even for such heavy seeds, we need to require a high duty cycle of BH growth at the Eddington accretion rate.…”

Section: Introductionmentioning

confidence: 99%

Super-Eddington growth of black holes in the early universe: effects of disc radiation spectra

Takeo

Inayoshi

Ohsuga

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the properties of accretion flows onto a black hole (BH) with a mass of M BH embedded in an initially uniform gas cloud with a density of n ∞ in order to study rapid growth of BHs in the early Universe. In previous work, the conditions required for super-Eddington accretion from outside the Bondi radius were studied by assuming that radiation produced at the vicinity of the central BH has a singlepower-law spectrum ν −α at hν ≥ 13.6 eV (α ∼ 1.5). However, radiation spectra surely depends on the BH mass and accretion rate, and determine the efficiency of radiative feedback. Here, we perform two-dimensional multi-frequency radiation hydrodynamical simulations taking into account more realistic radiation spectra associated with the properties of nuclear accretion disks. We find that the critical density of gas surrounding the BH, above which a transitions to super-Eddington accretion occurs, is alleviated for a wide range of masses of seed BHs (10 M BH /M 10 6 ) because photoionization for accretion disk spectra are less efficient than those for single-power-law spectra with 1 α 3. For disk spectra, the transition to super-Eddington is more likely to occur for lower BH masses because the radiation spectra become too hard to ionize the gas. Even when accretion flows are exposed to anisotropic radiation, the effect due to radiation spectra shrinks the ionized region and likely leads to the transition to a wholly neutral accretion phase. Finally, by generalizing our simulation results, we construct a new analytical criterion required for super-Eddington accretion; (M BH /10 5 M )(n ∞ /10 4 cm −3 ) 2.4 ( /100 eV) −5/9 , where is the mean energy of ionizing radiation from the central BH.

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Direct collapse black hole formation from synchronized pairs of atomic cooling haloes

Cited by 127 publications

References 42 publications

The emergence of the first star-free atomic cooling haloes in the Universe

The emergence of the first star-free atomic cooling haloes in the Universe

On the number density of ‘direct collapse’ black hole seeds

Super-Eddington growth of black holes in the early universe: effects of disc radiation spectra

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